Spectroscopic observation between 3-14 microns of 3 stars in
the TW Hya Association were obtained using the Aerospace
Corporation Broadband Array Spectrometer System (BASS) on
the NASA IRTF telescope. The targets observed were TW Hya,
HR 4796, and HD 98800. Both of the late-type stars, TW Hya
and HD 98800, exhibit a strong 10 micron silicate emission
band. The strong emission indicates the presence of small
dust grains close to the star, at angular distances not
currently accessible to coronagraphic techniques. The
spectral structure due to crystalline material that is
present in some young early-type stars (HD 163296, HD 31648,
etc.) is not apparent in these two objects. For HR 4796, the
dust emission is weak, but detectable above the expected
photospheric emission in the 10 micron band. The data are
unfortunately of insufficient quality for any detailed
mineralogical analysis.

This work was supported by the URC and Physics Department of
the University of Cincinnati (MLS), the Aerospace
Corporation IRD program (DKL and RWR), and the NOAO/STIS
project (CAG).